{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:DVVZPGAIOJOQT4ANZJN33IUCOR","short_pith_number":"pith:DVVZPGAI","schema_version":"1.0","canonical_sha256":"1d6b979808725d09f00dca5bbda2827473c8b845c57ceda3a232c598e90b32e1","source":{"kind":"arxiv","id":"1710.09882","version":2},"attestation_state":"computed","paper":{"title":"Are sdAs helium core stars?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"D. Koester, Ingrid Pelisoli, S. O. Kepler","submitted_at":"2017-10-26T19:26:06Z","abstract_excerpt":"Evolved stars with a helium core can be formed by non-conservative mass exchange interaction with a companion or by strong mass loss. Their masses are smaller than 0.5 MSun. In the database of the Sloan Digital Sky Survey (SDSS), there are several thousand stars which were classified by the pipeline as dwarf O, B and A stars. Considering the lifetimes of these classes on the main sequence, and their distance modulus at the SDSS bright saturation, if these were common main sequence stars, there would be a considerable population of young stars very far from the galactic disk. Their spectra are "},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1710.09882","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-10-26T19:26:06Z","cross_cats_sorted":[],"title_canon_sha256":"c0eb83345c40012cc60d72424055e09a2490a7c00994530977433179f20ab82d","abstract_canon_sha256":"d4cd453f327e4f7bc64c90967b6ce7ade7cc92625eb7f0d64a7a5f206c198b3b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:28:51.919017Z","signature_b64":"kIHsqbJYfKqjse1KD4qCyKNCu8NA7jihcjzKn2y+KuoBT/BxVlrBUrFU44H97bwwYuUnDdDcUZlW/U+9Yty0AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1d6b979808725d09f00dca5bbda2827473c8b845c57ceda3a232c598e90b32e1","last_reissued_at":"2026-05-18T00:28:51.918354Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:28:51.918354Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Are sdAs helium core stars?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"D. Koester, Ingrid Pelisoli, S. O. Kepler","submitted_at":"2017-10-26T19:26:06Z","abstract_excerpt":"Evolved stars with a helium core can be formed by non-conservative mass exchange interaction with a companion or by strong mass loss. Their masses are smaller than 0.5 MSun. In the database of the Sloan Digital Sky Survey (SDSS), there are several thousand stars which were classified by the pipeline as dwarf O, B and A stars. Considering the lifetimes of these classes on the main sequence, and their distance modulus at the SDSS bright saturation, if these were common main sequence stars, there would be a considerable population of young stars very far from the galactic disk. Their spectra are "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1710.09882","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1710.09882","created_at":"2026-05-18T00:28:51.918457+00:00"},{"alias_kind":"arxiv_version","alias_value":"1710.09882v2","created_at":"2026-05-18T00:28:51.918457+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1710.09882","created_at":"2026-05-18T00:28:51.918457+00:00"},{"alias_kind":"pith_short_12","alias_value":"DVVZPGAIOJOQ","created_at":"2026-05-18T12:31:12.930513+00:00"},{"alias_kind":"pith_short_16","alias_value":"DVVZPGAIOJOQT4AN","created_at":"2026-05-18T12:31:12.930513+00:00"},{"alias_kind":"pith_short_8","alias_value":"DVVZPGAI","created_at":"2026-05-18T12:31:12.930513+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.12242","citing_title":"Shaping the horizontal branch: The role of envelope mass in the evolution of stripped core-helium-burning stars","ref_index":16,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR","json":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR.json","graph_json":"https://pith.science/api/pith-number/DVVZPGAIOJOQT4ANZJN33IUCOR/graph.json","events_json":"https://pith.science/api/pith-number/DVVZPGAIOJOQT4ANZJN33IUCOR/events.json","paper":"https://pith.science/paper/DVVZPGAI"},"agent_actions":{"view_html":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR","download_json":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR.json","view_paper":"https://pith.science/paper/DVVZPGAI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1710.09882&json=true","fetch_graph":"https://pith.science/api/pith-number/DVVZPGAIOJOQT4ANZJN33IUCOR/graph.json","fetch_events":"https://pith.science/api/pith-number/DVVZPGAIOJOQT4ANZJN33IUCOR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR/action/storage_attestation","attest_author":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR/action/author_attestation","sign_citation":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR/action/citation_signature","submit_replication":"https://pith.science/pith/DVVZPGAIOJOQT4ANZJN33IUCOR/action/replication_record"}},"created_at":"2026-05-18T00:28:51.918457+00:00","updated_at":"2026-05-18T00:28:51.918457+00:00"}